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State of STAR

State of STAR. Outline : Data - Physics Detector Update Collaboration Update Physics Open Physics Issues Collaboration Issues Long Term Future. STAR Collaboration Meeting BNL 7 February 2002. John Harris. STAR. Data-Taken. Data Summer 2000 s nn = 130 GeV Au + Au

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State of STAR

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  1. State of STAR • Outline: • Data - Physics • Detector Update • Collaboration Update • Physics • Open Physics Issues • Collaboration Issues • Long Term Future STAR Collaboration Meeting BNL 7 February 2002 John Harris

  2. STAR Data-Taken Data Summer 2000snn = 130 GeV Au + Au  2.0 M total trigger events taken  844 K central (top 15%)  331 K (top 5%) central trigger events  458 K good minimum bias trigger events Data Fall 2001snn = 200 GeV Au + Au  ~ 14 M total trigger events taken  3.6 M (top 10%) central trigger events  4.7 M minimum bias trigger events Data Fall 2001 (1-day)snn = 20 GeV Au + Au  ~ 250 K total trigger events taken  30 K central trigger events  200 K minimum bias events Data Winter 2001-2s = 200 GeV p + p ~ 20 M total trigger events taken  17 M minimum bias trigger events for RHI reference data  subset with forward pi-zero trigger (single spin asymmetry)

  3. Data on tape Min Bias events = 10x more than last year Central events = 7x more than last year Physics Reach High-pt h spectra and anisotropy out to 12 GeV/c ratios at high-pt (RICH) Strangeness ,  (width, mass-shifts), higher reach in pT for (multi-) strange baryons, (1520), K*(1430), (1385) HBT 3D K-K, K- w/ greater resolution, K-p, -p, K0s-K0s, pt dependence of R() Spectra , He4, particle ratio EbyE , K* flow, K/ … and much more … (also p + p reference data and spin surprises) STAR What Physics to Expect from 2001 Au + Au Run

  4. Status of the Detector at RHIC Silicon Vertex Tracker + Silicon Strip Detector Coils Magnet EM Cal Barrel + End Cap EMC Time Projection Chamber Trigger Barrel + Time of Flight Patch Ring Imaging Cerenkov Detector Electronics Platforms STAR Forward Time Projection Chamber “Large acceptance hadronic detector” Detectors Run 2000 • TPC, Trigger Barrel, RICH Detector Installation 2002: • SSD, PMD,  1/2 EMC, move RICH, EEMC (?) New Detectors 2001 Run: • SVT, FTPCs, ToF patch, partial EMC, FPD, BBC

  5. STAR Status of the Collaboration BrazilRussia Universidade de Sao Paolo MEPHI – Moscow LPP/LHE JINR - Dubna China IHEP-Protvino IHEP - Beijing USTC - Hefei IMP - Lanzhou SINR - Shanghai Tsinghua University IPP - Wuhan U.S. Labs Argonne National Laboratory EnglandBrookhaven National Laboratory University of Birmingham Lawrence Berkeley National Laboratory FranceU.S. Universities IReS Strasbourg UC Berkeley / SSL SUBATECH - Nantes UC Davis UC Los Angeles GermanyCarnegie Mellon University MPI – Munich Creighton University University of Frankfurt Indiana University Kent State University India Michigan State University IOP - Bhubaneswar City College of New York VECC - Calcutta Ohio State University Panjab University Penn. State University University of Rajasthan Purdue University Jammu University Rice University IIT - Bombay University of Texas - Austin Texas A&M University Poland University of Washington Warsaw University of Technology Wayne State University Yale University 419 collaborators 44 institutions 9 countries

  6. STAR Physics Progress: Conclusions So Far •  low net baryon density  approaches early Universe •  particle ratios  consistent with quark coalescence •  strong radial and elliptic flow large pressure gradients •  simple models of radial flow “fit” spectra [ definitely too naïve? ] Kinetic parameters: ßr (RHIC) = 0.6c , Tfo (RHIC) = 100-120 MeV • Do not yet understand details of flow or expansion!! •  simple chemical model “fits” ratios [ fundamental or too naïve? ] Chemical parameters: Tch (RHIC) = 175 MeV , B (RHIC) = 51 MeV • Need multiply strange baryon data for hard test!! •  source sizes similar to SPS inconsistent with hydrodynamical models • Do not yet understand spacetime evolution!! •  variables wrt flow plane! further constrain dynamical models  single particle distributions and elliptic flow at high Pt  most exciting data at QM  parton energy loss in-medium? • Need pp and pA reference data to understand mechanisms!!

  7. STAR Physics Progress: STAR Journal Publications/Submissions • Midrapidity f-meson Production in Au+Au at snn = 130 GeVsubmitted to Phys. Rev. C • Measurement of Inclusive Anti-Protons from Au+Au at snn = 130 GeV C. Adler et al. Phys. Rev. Lett. 87, 262302-1 (2001). • Anti-deuteron and Anti-helium3 Production in Au+Au at snn = 130 GeV C. Adler et al. Phys. Rev. Lett. 87, 262301-1 (2001). • Identified Particle Elliptic Flow in Au+Au at snn = 130 GeVC. Adler et al. Phys. Rev. Lett. 87, 182301 (2001). • Multiplicity Distribution and Spectra of Negatively Charged Hadrons in Au+Au at snn = 130 GeV C. Adler et al. Phys. Rev. Lett. 87, 112303 (2001). • Pion Interferometry of snn = 130 GeV Au+Au at RHICC. Adler et al. Phys. Rev. Lett. 87, 082301 (2001). • Midrapidity Antiproton-to-Proton Ratio from Au+Au snn = 130 GeVC. Adler et al. Phys. Rev. Lett. 86, 4778 (2001). • Elliptic Flow in Au+Au at snn = 130 GeV K.H. Ackermann et al. Phys. Rev. Lett. 86, 402 (2001).

  8. Physics in Progress STAR STAR Physics Papers in Preparation from 130 GeV Au + Au • Spectra Midrapidity Inclusive p and pbar* Particle Production Summary Paper (PRC) Pi-zero Paper (PRC) • Strangeness • Cascade Paper • Mixed Hadron Ratio Paper (PRC) • High pt • Inclusive High Pt Spectra and V2 Paper(s) • Event-by-Event • Multiplicity Fluctuations Paper* (PRC) • Balance Functions* (PRL) + • Pt Fluctuations Paper (2) in Special Committee • 4-Particle Correlation Paper* (PRC) + • HBT • 3-pion Correlations* (PRL) + • K-pi Correlations* (PRL) + • Phase Space Density • Azimuthally Sensitive HBT* (PRL) • Ultra-Peripheral Collisions • Production of the r-meson in UPC • In Godfather Committee: • Ratios Paper (PRL) • K* Paper (PRL) • Strange Particle Flow (PRL) • Kaon Paper • ~ ready for submission: • Lambda Paper * = completed preview

  9. STAR PWG Convenor Group Paper Preview Process • PWG Convenor (PWGC) Group agreed to meet: • - bi-weekly meetings by telephone. • - in-person 1 day/month to discuss PWGC business. • - Physics Analysis Coordinator (PAC) will chair these meetings. • In order to: • 1) allow early examination of "papers" by a group with a broad physics perspective and a range of individual physics interests in STAR. This could include the merging of different types of analyses, specific figures, and possibly papers. This will rapidly become important for STAR as we attempt to correlate our results and better understand the physics from our data. We also anticipate that more "interpretive" papers, including a range of data and analyses from STAR, will become increasingly important. Such an early overview of proposals will help STAR prepare and publish better papers. • 2) provide guidance on the journal for which each paper is targeted, and • 3) provide feedback and guidance to the PA's and PWG Convenors before the text and format of papers have been determined. Early examination is important to allow direction changes prior to any large investment of time and effort on the text of papers.

  10. STAR PWG Convenor Group Paper Preview Process Spokesman & Physics Working Group Convenor Group decided unanimously: - to institute practice of Principal Authors submitting proposals for papers to the Spokesman, once the analysis has been discussed in the PWG and agreed to be sound, but prior to agreement on the text. - proposal to include abstract primary physics points of the paper proposed figures and tables other supporting or explanatory info journal to which paper is intended for submission. Physics Analysis Coordinator and the PWGC Group are charged to discuss each proposal and make recommendations on proposal to the Spokesman. Spokesman shall provide PA's and PWG Convenors with relevant PWGC Group's guidance on proposal. This is intended to be a fast process. Presented to Council (Dec. 7) / will be discussed tomorrow also.

  11. STAR Physics - “accomplished a lot, much more to do, so little beam time!” • What are the open questions? • Deconfinement? • Chiral restoration? • Understand Dynamics (early, expansion, late stages) & kinetic properties • Parton Propagation (systematics, Cronin, propagation in hadronic matter) • What must we still measure? When (next slide)? • Multiply-strange baryon spectra (s and A dependences) • J/y  e+e- • Open Charm (D-mesons)  future • Disoriented chiral condensates? low Pt spectra, charge/neutral ratios • F e+e- • Particle production systematics • Evolution (and systematics) of colliding systems • High Pt hadrons (at least to 10 - 12 GeV/c, other systems inc. p/d + Au) • also p, p out to 5 GeV/c • High Pt correlations future • Still Room for New Ideas! • Photon-Pomeron Physics! • Entire Spin Physics Program!

  12. STAR RHI Physics Program 2001 - 2005 Relativistic Heavy Ion Physics (AA plus reference data using pp, pA) Soft (pt < 2 GeV/c) Physics (2000 - 2004) • identified particle spectra (p, K, p, anti-particles, strange particles, resonances) • light anti-nuclei yields • flow • particle correlations • multiply-strange baryon (X, W) spectra • transverse energy production • event-by-event fluctuations (inc: charge, DCC, pt , ...; P, CP violations) • studies of event classes High pt Physics (2000 - 2004) • parton energy loss • charged single particles • identified particles (inc. po) to ~ 5 GeV/c • high pt particle correlations, photons, jets* “electrons” (2002/3 ) • f  e+e- • J/y  e+e- p/d + A physics (2002 ) • nuclear structure functions/shadowing (g-jet) • jets, direct photons • J/y  e+e-

  13. STAR Photon/Pomeron Physics and Spin Physics Programs 2001 - 2005 Photon/Pomeron Physics (ultra-peripheral AA) Two-photon and photon-pomeron physics (2000 - 2003) • states with mass < 2 GeV (2-prong final states) • multiple vector meson production (4-prong final states) • J/y  e+e- Higher mass states (2002/3 ) • electron decays of higher charm states • final states containing photons • particle identification to identify higher mass strange and charm decays • trigger on semi-leptonic decays of charm states • …. Spin physics(2001  2005) 2001 AN (with transverse spin) 2002  start (?) to measure ALL via inclusive jet production  sensitive to DG 2003  measure ALL via direct photons and jets  sensitive to DG DG(x) and Dq(x) from dijet production Higher energy - tests of parity-violating asymmetries in W production 2004  ALL from g-jet coincidences ALL from Drell-Yan production of e+e- Initial studies of parity-violating asymmetries in W production 2005  Measurement of parity-violating asymmetries in W production (quark and anti-quark contribution to proton spin)

  14. STAR Summary Detector Additions 2001 - 2004 • STAR Installation for 2001 Run • Silicon Vertex Tracker • Barrel Electromagnetic Calorimeter modules (complete 24 of 120 modules) • Level 3 Processors • 2 Forward Time Projection Chambers • Time-of-Flight Patch • STAR Installation for 2002 Run • Silicon Strip Detector • Barrel Electromagnetic Calorimeter modules (complete 60 of 120) • Endcap Electromagnetic Calorimeter (lower half installed) • Data Rate Increase • Level 1,2,3 Processors • STAR Installation for 2003 Run • Barrel Electromagnetic Calorimeter modules (complete 88 of 120) • Endcap Electromagnetic Calorimeter (complete, 1 < h < 2, Df = 2p)) • Photon Multiplicity Detector • start Time-of-Flight Barrel? • STAR Installation for 2004 Run • Barrel Electromagnetic Calorimeter modules (complete 120 of 120. I.e. -1 < h < 1, Df = 2p) • Time-of-Flight Barrel (completed in 2005)? • start Micro-vertex Detector?

  15. STAR Issues in STAR • “Physics First!” • detectors  data-taking  recon  analysis  papers • “complex” convergence • Physics, physics directions, and future • open discussion • common goals  guidance (Spokesperson, Council, Collaboration) • Sociology • individuals working toward common goals • representation and voice • diversify committees (Talks, PWGC Group, GFCs,…) • service work • inclusive

  16. STAR Future of STAR • Finish papers for snn= 130 GeV Au + Au • esp. High Pt, Strange baryons, ………………… • Start snn= 200 GeV Au + Au, p + p production, and analyse for physics • physics for Quark Matter………beyond • Must increase data (for-physics) rates • continue to increase • trigger capabilities (to select physics of interest) • (Trigger Board is in place) • DAQ rates • cpu/disk for recon/analysis • install and commission new detectors • EMC, SSD, PMD, TOF-RPC patch, …TOF-barrel……mvtx…..) • test, install and commission new software • Integrated Tracking • R&D and Detector Plans (see afternoon session) • STAR Future Physics Workshop in April (details in Ludlam’s talk) • Decide STAR Physics Goals & Priorities (this summer) • Determine R&D Funding Requests (this summer) • Must finally get STAR Detector Trailer at STAR Hall! • Long Term Major Upgrade Proposal (end of year)

  17. The End

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